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T1 - Synthesis of the elements in stars

At this temperature, nucleosynthesis, or the production of light elements, could take place.

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Nucleosynthesis: The Formation of Elements in the …

In 1939, in a paper entitled "Energy Production in Stars", Hans Bethe analyzed the different possibilities for reactions by which hydrogen is fused into helium. He selected two processes that he believed to be the sources of energy in stars. The first one, the proton-proton chain, is the dominant energy source in stars with masses up to about the mass of the Sun. The second process, the carbon-nitrogen-oxygen cycle, which was also considered by Carl Friedrich von Weizsäcker in 1938, is most important in more massive stars. These works concerned the energy generation capable of keeping stars hot. They did not address the creation of heavier nuclei, however. That theory was begun by Fred Hoyle in 1946 with his argument that a collection of very hot nuclei would assemble into iron. Hoyle followed that in 1954 with a large paper outlining how advanced fusion stages within stars would synthesize elements between carbon and iron in mass.

Synthesis of Elements | SpringerLink

I think that this aspect—transformation—adds an additional layer of cool beyond just common origin. In one sense, stellar nucleosynthesis represents an important example of the ability of simple mechanisms to produce complex results. In this case, heat and gravity over time have been enough to produce all of the elements needed for life to develop on Earth. It’s a hidden premise in many minds that complexity can only come from more complexity. Stellar nucleosynthesis is an elegant and direct example of exactly the opposite.

Neutron capture and stellar synthesis of heavy elements.

Neutron capture and stellar synthesis of heavy elements

Near the end of its life, a star will fuse carbon and helium to form oxygen. Very large stars—those larger than eight times the size of our own sun—even have enough gravity to fuse carbon, producing neon, magnesium and other elements. In those stars, when the carbon has been exhausted, gravity may provide enough energy for neon and oxygen to fuse. This phase doesn’t last long; a star may fuse all its available oxygen in a year, leaving little besides silicon and sulfur. During the last 24 hours of its life, the star fuses its silicon, producing large quantities of nickel and iron and smaller quantities of some other elements. This is the bottom of the hill for “ordinary” stellar nucleosynthesis—and it’s the source of all the oxygen, carbon, iron, nickel, silicon and other common elements in the universe.

Most of the things in our “Treasures” series are living organisms. I think this is partly because lots of living organisms are easy to identify with: they exist on a scale similar to ours and are easy to categorize as discrete entities. Phenomena are a little harder to sell, for the most part. Stellar nucleosynthesis has had some help though, in the form of Carl Sagan’s wildly popular and surprisingly durable . And it’s true: we’re literally made of atoms that came here from dying stars. Of course this is equally true of centipedes, norovirus and Rob Ford, so admittedly the magic relies on a bit of anthropocentrism.

GSI - Synthesis of Heavy Elements

Importance of the photo-beta process for the synthesis of “p” elements in stellar conditions

N2 - Forty years ago Burbidge, Burbidge, Fowler, and Hoyle combined what we would now call fragmentary evidence from nuclear physics, stellar evolution and the abundances of elements and isotopes in the solar system as well as a few stars into a synthesis of remarkable ingenuity. Their review provided a foundation for forty years of research in all of the aspects of low energy nuclear experiments and theory, stellar modeling over a wide range of mass and composition, and abundance studies of many hundreds of stars, many of which have shown distinct evidence of the processes suggested by B2FH. In this review we summarize progress in each of these fields with emphasis on the most recent developments.

AB - Forty years ago Burbidge, Burbidge, Fowler, and Hoyle combined what we would now call fragmentary evidence from nuclear physics, stellar evolution and the abundances of elements and isotopes in the solar system as well as a few stars into a synthesis of remarkable ingenuity. Their review provided a foundation for forty years of research in all of the aspects of low energy nuclear experiments and theory, stellar modeling over a wide range of mass and composition, and abundance studies of many hundreds of stars, many of which have shown distinct evidence of the processes suggested by B2FH. In this review we summarize progress in each of these fields with emphasis on the most recent developments.

The subsequent nucleosynthesis of the elements (including all ..
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  • Synthesis of the Elements in Stars | SpringerLink

    11/12/1970 · Synthesis of the Elements in Stars

  • Synthesis of the elements in stars: forty years of progress

    The Synthesis of the Elements ..

  • The Synthesis of the Elements: ..

    Stellar nucleosynthesis is within the scope of WikiProject Astronomy, ..

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Periodic Table Database | Chemogenesis

Modern stellar population synthesis assumes that the stellar populationsin galaxies consist of a sum of ,building blocks of more complex stellar populations, entities thatconsist of all stars born at the same time, with the samemetallicity.

Nuclear Reactions in Stars - Georgia State University

STELLAR POPULATION MODELS AND THEIR INGREDIENTSWith stellar population synthesis one wants to determine as muchinformation from the stellar populations of an unresolved galaxy from asingle spectrum as possible.

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However, one knows that different types ofsupernovae produce different relative fractions of elements: forexample, since the rate of element production depends on stellar mass,the relative distribution of elements ejected into the ISM in a SNexplosion must also depend on mass.

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So there's one major difference between the two universes in terms of elemental composition.

The stellar forge will follow the basic premise that is reflected in the chart: that older stars will have fewer heavy metallic elements than younger stars, because the younger stars are forming out of the gas clouds that have been contaminated by the older stars exploding and releasing those elements.

But in terms of specifically tying element probability to star type, no, I seriously doubt the stellar forge has that programmed into it.

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But does the Stellar Forge follow this formula?

Are you questioning the distribution of elements (mined and extracted for engineers) in relation to local sources?

The chemical composition of a star system typically depends on the matter cloud that the system accretes from and that cloud depends upon the age, size, class and generation of the star which exploded/dissipated before hand to determine its element zoo ratios.

For the sake of a game, Stella forge would need to think back a stella generation before rendering the galaxy seen in the game.

I understand where elements come from and how they are created but i can honestly say that its never been a factor for me in ED whether or not the elements found and there ratios seem appropriate for the setting.

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